This model from Nandra et al. (2007) combines pexrav with self-consistently generated Fe K, Fe K, Ni K and the Fe K Compton shoulder. Line strengths are based on Monte Carlo calculations by George & Fabian (1991) which are parametrized for by :
with inclination dependence for degrees :
and abundance dependence :
The Fe K and Ni K line fluxes are 11.3% and 5% respectively of that for Fe K. The Fe K Compton shoulder is approximated as a gaussian with E = 6.315 keV and keV. The inclination dependence is taken from Matt (2002) such that :
The model parameters are :
par1 | , power-law photon index, . |
par2 | , cutoff energy in keV (if = 0 there is no cutoff). |
par3 | scale, the scaling factor for reflection; <0 = no direct component, 1 = isotropic source above the disk |
par4 | , redshift |
par5 | , abundance of elements heavier than He relative to Solar. |
par6 | , iron abundance relative to Solar. |
par7 | the inclination angle (degrees). |
norm | normalization is the photon flux at 1 keV (photons/keV/cm/s) of the cutoff power law only (without reflection) and in the Earth frame. |